Abstract
Some recent results are reviewed that lead us now to believe that accretion discs are basically always magnetised. The main components are Balbus-Hawley and Parker instabilities on the one hand and a dynamo process on the other. A mechanical model for the Balbus-Hawley instability is presented and analysed quantitatively. Three-dimensional simulations are discussed, especially the resulting magnetic field structure. Possibilities of reproducing the field by an αΩ dynamo are investigated, especially its symmetry with respect to the midplane.
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Brandenburg, A., Campbell, C. (1997). Modelling magnetised accretion discs. In: Meyer-Hofmeister, E., Spruit, H. (eds) Accretion Disks — New Aspects. Lecture Notes in Physics, vol 487. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0105826
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DOI: https://doi.org/10.1007/BFb0105826
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